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The structure of AGNs from X-ray eclipses

The structure of AGNs from X-ray eclipses . Guido Risaliti (CfA & INAF-Arcetri). M. Salvati, E. Nardini (INAF-Arcetri) , R. Maiolino (INAF-Roma) , G. Matt, S. Bianchi (Roma3) , V. Braito (Leicester) , M. Elvis, G. Fabbiano, (CfA). Ubiquitous Variability of N H in Seyfert Galaxies.

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The structure of AGNs from X-ray eclipses

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  1. The structure of AGNs from X-ray eclipses Guido Risaliti (CfA & INAF-Arcetri) M. Salvati, E. Nardini (INAF-Arcetri), R. Maiolino (INAF-Roma), G. Matt, S. Bianchi (Roma3), V. Braito (Leicester), M. Elvis, G. Fabbiano, (CfA)

  2. Ubiquitous Variability of NH in Seyfert Galaxies NH variable in 23/25 sources Timescales from months to years Clumpy absorber Sub-parsec distance Risaliti, Elvis & Nicastro 2002 Leicester - Jan 04, 2009

  3. Ubiquitous Variability of NH in Seyfert Galaxies Common also on short time scales! (~10 sources with confirmed occultations in hours-days) • Method: • * Detection of candidate occultations • * Confirmation through spectral analysis • Applications: • * Physical parameters of the X-ray source and the X-ray absorber • * Hints on the geometrical structure of the absorbing clouds • * Shape of the absorbing clouds • * POSSIBLE EXPERIMENT OF DISK TOMOGRAPHY

  4. Method: XMM long look of Mrk 766

  5.  No absorption, “standard” model  NH~1023cm-2, C.F. ~ 80% No continuum spectral variation

  6. Ubiquitous Variability of NH in Seyfert Galaxies Eclipses on short time scales are common ! (~10 sources with confirmed occultations in hours-days) (Risaliti et al. 2010)

  7. Finding more sources with eclipses in ~hours-days NGC 4388 NGC 4151 DNH~2*1023 cm-2 DT~15 hours DNH~3*1023 cm-2 DT<15 days DNH~1023 cm-2 DT~2 days UGC 4203 NGC 7582 DNH~1023 cm-2 DT~20 hours (Bianchi et al. 2009)

  8. General results: Eclipses of the X-ray source are COMMON in nearby AGN DNH ~ 1023-1024cm-2 V > 103 km/s D ~ 1013 cm n ~ 1010-1011 cm-2 X-ray absorber = BLR clouds X-ray source size ~ a few RG

  9. Structure of the absorber HR NGC 1365 Suzaku NH CF Maiolino et al. 2010

  10. Tomography of the X-ray source A Relativistic Iron Line in NGC 1365 (Risaliti et al. 2009) • It is really a relativistic line • Long look (>300 ks) • Source in Compton-thin state • Complete 10-hours C-thick eclipse during obs. Assumptions:

  11. Simulation: IXO observation of the eclipsing iron line IXO

  12. Simulation: XMM observation of the eclipsing iron line

  13. IXO observation of the already observed eclipses blue red blue red blue red blue red

  14. CONCLUSIONS • Variability on short time scales is common in local AGNs •  X-ray absorber == BLR clouds •  Size of the X-ray source ~ a few RG • Detailed analysis of the highest S/N X-ray eclipses: •  “Cometary” shape of clouds • Possible tests of GR effects & disk tomography

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